Y. Doi, T. Hasegawa, R. S. Furuya, S. Coudť, C. L. H. Hull, D. Arzoumanian, P. Bastien, M. C.-Y. Chen, J. Di Francesco, R. Friesen, M. Houde, S.-I. Inutsuka, S. Mairs, M. Matsumura, T. Onaka, S. Sadavoy, Y. Shimajiri, M. Tahani, K. Tomisaka, C. Eswaraiah, P. M. Koch, K. Pattle, C. Won Lee, M. Tamura, D. L. Berry, T.-C. Ching, J. Hwang, W. Kwon, A. Soam, J.-W. Wang, S.-P. Lai, K. Qiu, D. Ward-Thompson, D.-Y. Byun, H.-R. V. Chen, W. P. Chen, Z. Chen, J. Cho, M. Choi, Y. Choi, A. Chrysostomou, E. J. Chung, P. N. Diep, H.-Y. Duan, L. Fanciullo, J. Fiege, E. Franzmann, P. Friberg, G. Fuller, T. M. Gledhill, S. F. Graves, J. Greaves, M. Griffin, Q. Gu, I. Han, J. Hatchell, S. S. Hayashi, T. Hoang, T. Inoue, K. Iwasaki, I.-G. Jeong, D. Johnstone, Y. Kanamori, J.-h. Kang, M. Kang, S.-j. Kang, A. Kataoka, K. S. Kawabata, F. Kemper, G. Kim, J. Kim, K.-T. Kim, K. H. Kim, M.-R. Kim, Shinyoung Kim, J. M. Kirk, M. I. N. Kobayashi, V. KŲnyves, T. Kusune, J. Kwon, K. Lacaille, C.-Y. Law, C.-F. Lee, H. Lee, J.-E. Lee, S.-S. Lee, Y.-H. Lee, D. Li, D. Li, H.-b. Li, H.-L. Liu, J. Liu, S.-Y. Liu, T. Liu, I. De Looze, A. -R. Lyo, B. C. Matthews, G. H. Moriarty-Schieven, T. Nagata, F. Nakamura, H. Nakanishi, N. Ohashi, G. Park, H. Parsons, N. Peretto, T. S. Pyo, L. Qian, R. Rao, M. G. Rawlings, B. Retter, J. Richer, A. Rigby, H. Saito, G. Savini, A. M. M. Scaife, M. Seta, H. Shinnaga, Y.-W. Tang, Y. Tsukamoto, S. Viti, H. Wang, A. P. Whitworth, H.-W. Yen, H. Yoo, J. Yuan, H.-S. Yun, T. Zenko, C.-P. Zhang, G. Zhang, Y. Zhang, J. Zhou, L. Zhu, Ph. Andrť, C. D. Dowell, S. Eyres, S. Falle, S. van Loo, J.-F. Robitaille
We present new observations of the active star formation region NGC 1333 in the Perseus molecular cloud complex from the James Clerk Maxwell Telescope B-Fields In Star-forming Region Observations (BISTRO) survey with the POL-2 instrument. The BISTRO data cover the entire NGC 1333 complex (~1.5 pc × 2 pc) at 0.02 pc resolution and spatially resolve the polarized emission from individual filamentary structures for the first time. The inferred magnetic field structure is complex as a whole, with each individual filament aligned at different position angles relative to the local field orientation. We combine the BISTRO data with low- and high- resolution data derived from Planck and interferometers to study the multiscale magnetic field structure in this region. The magnetic field morphology drastically changes below a scale of ~1 pc and remains continuous from the scales of filaments (~0.1 pc) to that of protostellar envelopes (~0.005 pc or ~1000 au). Finally, we construct simple models in which we assume that the magnetic field is always perpendicular to the long axis of the filaments. We demonstrate that the observed variation of the relative orientation between the filament axes and the magnetic field angles are well reproduced by this model, taking into account the projection effects of the magnetic field and filaments relative to the plane of the sky. These projection effects may explain the apparent complexity of the magnetic field structure observed at the resolution of BISTRO data toward the filament network.
Interstellar medium; Interstellar magnetic fields; Interstellar filaments; Star formation; Polarimetry; Submillimeter astronomy
The Astronomical Journal
Volume 899, Number 1